15 March 2012

Measurement of the neutrino velocity with the ICARUS detector at the CNGS beam

M. Antonelloa, P. Aprilia, B. Baibussinovb, M. Baldo Ceolinb,✝, P. Benettic,

E. Calligarichc, N. Cancia, F. Carbonarad, S. Centrob, A. Cesanaf, K. Cieslikg, D. B. Clineh, A.G. Coccod, A. Dabrowskag, D. Dequalb, A. Dermenevi, R. Dolfinic,

C. Farneseb, A. Favab, A. Ferrarij, G. Fiorillod, D. Gibinb, A. Gigli Berzolaric,✝, S. Gninenkoi, A. Guglielmib, M. Haranczykg, J. Holeczekl, A. Ivashkini, J. Kisiell,

I. Kochanekl, J. Lagodam, S. Manial, G. Mannocchin, A. Menegollic, G. Mengb, C. Montanaric, S. Otwinowskih, L. Perialen, A. Piazzolic, P. Picchin,

F. Pietropaolob, P. Plonskio, A. Rappoldic, G.L. Rasellic, M. Rossellac, C. Rubbiaa,j, P. Salaf, E. Scantamburloe, A. Scaramellif, E. Segretoa, F. Sergiampietrip,

D. Stefana, J. Stepaniakm, R. Sulejm,a, M. Szarskag, M. Terranif, F. Varaninib, S. Venturab, C. Vignolia, H. Wangh, X. Yangh, A. Zalewskag, K. Zarembao.

(ICARUS Collaboration) and

P. Alvarez Sanchezj .J. Serranoj (CERN, Geneva, Switzerland)

a Laboratori Nazionali del Gran Sasso dell'INFN, Assergi (AQ), Italy b Dipartimento di Fisica e INFN, Università di Padova, Via Marzolo 8, I-35131

Padova, Italy c Dipartimento di Fisica Nucleare e Teorica e INFN, Università di Pavia, Via

Bassi 6, I-27100 Pavia, Italy d Dipartimento di Scienze Fisiche, INFN e Università Federico II, Napoli, Italy e Dipartimento di Fisica, Università di L'Aquila, via Vetoio Località Coppito, I-

67100 L'Aquila, Italy f INFN, Sezione di Milano e Politecnico, Via Celoria 16, I-20133 Milano, Italy g Henryk Niewodniczanski Institute of Nuclear Physics, Polish Academy of

Science, Krakow, Poland h Department of Physics and Astronomy, University of California, Los Ange-

les, USA i INR RAS, prospekt 60-letiya Oktyabrya 7a, Moscow 117312, Russia j CERN, CH-1211 Geneve 23, Switzerland k Institute of Theoretical Physics, Wroclaw University, Wroclaw, Poland l Institute of Physics, University of Silesia, 4 Uniwersytecka st., 40-007 Katowi-

ce, Poland m National Centre for Nuclear Research, A. Soltana 7, 05-400 Otwock/Swierk,

Poland n Laboratori Nazionali di Frascati (INFN), Via Fermi 40, I-00044 Frascati, Italy o Institute of Radioelectronics, Warsaw University of Technology,

Nowowiejska, 00665 Warsaw, Poland p INFN, Sezione di Pisa. Largo B. Pontecorvo, 3, I-56127 Pisa, Italy ✝ Deceased

2

Abstract

The CERN-SPS accelerator has been briefly operated in a new, lower in-tensity neutrino mode with ~1012 p.o.t. (protons on target)/pulse) and with a beam structure made of four LHC-like extractions, each with a narrow width of ~3 ns, separated by 524 ns (1/4 of the proton revolution time in the CERN-PS). This very tightly bunched beam structure represents a substantial progress with respect to the ordinary operation of the CNGS beam, since it allows a very ac-curate time-of-flight measurement of neutrinos from CERN to LNGS on an event-to-event basis.

The ICARUS T600 detector (CNGS2) has collected 7 beam-associated events, consistent with the CNGS delivered neutrino flux of 2.2 x 1016 p.o.t. and in agreement with the well known characteristics of neutrino events in the LAr-TPC.

The time of flight difference δt between the speed of light and the arriv-ing neutrino LAr-TPC events has been analysed. The result is compatible with the simultaneous arrival of all events with equal speed, the one of light,

€

δt = 0.3 ± 4.0stat ± 9.0syst( ) ns. This is in a striking difference with the reported re-sult of OPERA [1] that claimed that high energy neutrinos from CERN should arrive at LNGS about 60 ns earlier than expected from luminal speed.

3 1 Introduction

The OPERA collaboration has recently announced the measurement of the velocity of neutrinos, as they travel from CERN to the Gran Sasso Laborato-ry (LNGS) covering a distance of about 730 km [1]. OPERA (CNGS1) reported the surprising result that neutrinos arrive earlier than expected from luminal speed by a time interval δt = 57.8±7.8(stat.) −5.9

+8.3(syst.)( ) ns . This corresponds to a superluminal propagation speed of neutrinos of an amount δcν = 2.37±0.32(stat.) −0.24

+0.34(syst.)( )×10−5 , where

€

δcν ≡ vν − c( ) c . MINOS [2] had previously performed a similar measurement after a distance of 735 km and a neutrino spectrum with an average energy of 3 GeV. Although less significant statistically, the corresponding MINOS result is

€

δcν = 5.1± 2.9( ) ×10−5 at 68% C.L. This measurement is consistent with the speed of light to less than 1.8σ. The corresponding 99% confidence interval on the speed of the neutrino is

€

−2.4 ×10−5 ≤ δcν ≤12.6 ×10−5 . Earlier experiments [3] had set upper limits of

about

€

δcν ≤ 4 ×10−5 in the energy range 30 to 300 GeV.

The OPERA result has triggered new experimental determinations, since — if confirmed — it will call for a complete reconsideration of the basic princi-ples of particle physics. Cohen and Glashow [4] have argued that such super-luminal neutrinos should lose energy by producing photons and

€

e+e−pairs, through ZO mediated processes, analogous to Cherenkov radiation. In the same LNGS neutrino beam from CERN, the ICARUS collaboration (CNGS2) [5-7] has recently experimentally searched for superluminal Cherenkov-like

€

e+e−pairs inside the fiducial volume of its large TPC-LAr detector [8]. No candidate event was found, setting a tight negative limit

€

δcν ≤ 2.5 ×10−8 at 90% confidence level.

The limit for the Cohen and Glashow effect at our energies is therefore compa-rable to the limit of

€

δcν ≡ vν − c( ) c from the lower energy SN1987a [9-12].

In order to initiate a new campaign of measurements on the neutrino time of flight, from October 21st to November 6th 2011, the CERN-SPS accelera-tor has been operated in a new, lower intensity mode with ~1012 p.o.t (protons on target) and with a beam structure made of four LHC-like extractions, each with a narrow width of ~3 ns, separated by 524 ns (1/4 of the proton revolution time in the CERN-PS). This very tightly bunched beam structure represents a substantial progress since it allows a very accurate neutrino time-of-flight measurement on an event-to-event basis.

Experimental data have been collected by CNGS1 (OPERA) and CNGS2 (ICARUS) neutrino dedicated experiments, as well as by other experiments at LNGS. We hereby report the experimental observation of the neutrino velocity distribution of the events observed in ICARUS, combining the accurate deter-mination of the distance and time of flight with the direct observation of either neutrino events inside the detector or of neutrino associated muons from the surrounding rock. Recent, high-accuracy GPS measurements and optical trian-

4

gulations have provided us with a determination of the distance from CERN to LNGS and up to the ICARUS detector with an uncertainty of centimetres and with an upgraded GPS-based timing system at CERN and LNGS with uncer-tainties of a few nanoseconds.

Based on seven neutrino events, our result is in excellent agreement with Lorentz dependent velocities of neutrinos and of light. Neutrinos and GPS measurements are found to be sharply coincident in time within an uncertainty of a few nanoseconds, in disagreement with the superluminal result reported by the OPERA Collaboration [1].

2 Synchronizing between CERN and LNGS

A detailed description of the CERN and LNGS timing systems and their synchronizations are given in Ref. [1] and Ref. [13]. A schematic picture of the timing systems layout, including all timing delays is shown in Figure 1. The origin of the neutrino velocity measurement is referred to the Beam Current Transformer (BCT) detector (BFCTI.400344), located 743.391 ± 0.002 m upstream of the CNGS neutrino target.

The proton beam time-structure at the BCT is recorded by a 1 GS/s Wave Form Digitiser (WFD) ACQIRIS DP110 triggered by the kicker magnet signal. The BCTFI.400344 waveform for every extraction is stored into the CNGS database. Every acquisition is time-tagged with respect to the SPS timing system, associating each neutrino event at LNGS to a precise proton bunch.

The absolute UTC timing signal at LNGS is provided every second (PPS) by a GPS system ESAT 2000 disciplined with a Rubidium oscillator [14, 15], op-erating on the surface Laboratory. A copy of this signal is sent underground every ms (PPmS) and used in ICARUS to provide the absolute time-stamp to the recorded events.

In order to improve the ~100 ns time accuracy of the standard GPS at CERN and LNGS, the OPERA collaboration and CERN have installed, both at CERN and LNGS, two new identical systems composed of a GPS receiver for time-transfer applications Septentrio PolaRx2e operating in “common-view” mode and a Cs atomic clock Symmetricom Cs4000 [1].

The Cs4000 oscillator provides the reference frequency to the PolaRx2e receiver, and a CTRI device logs every second the difference in time between the 1PPS outputs of the standard GPS receiver and of the more precise Po-laRx2e, with 0.1 ns resolution. The residual time base fluctuations between the CERN and the LNGS PolaRx2e receivers introduces a systematic error of ~ 1.0 ns. The stability of this calibration was recently confirmed [1].

5

The timing signal (PPmS), distributed by the LNGS laboratory, consists of a TTL positive edge (15 ns rise time) sent out every ms and followed, after 200 µs, by the coding of the absolute time related to the leading edge. This sig-nal is generated in the external laboratory and sent to the underground hall B via ~ 8 km fiber optics. This introduces a delay of 42036.6 ± 1.3 ns, accurately calibrated in December 2011, following a double path procedure very similar to the one devised by the OPERA experiment for their first calibration in 2006 [1].

The method consists in measuring the time difference ∆t and time sum Σt of the signal propagation along the usual path and an alternative one using a spare fibre.

1. In the first configuration the 1PPS output of the ESAT-2000 GPS receiver was converted into an optical signal, sent underground via the spare fi-bre and converted back into electrical. The difference in the propagation delays, between this signal and the 1PPmS output of the ESAT-2000 GPS propagated over the standard path, was measured underground taking as a reference the middle height of the rising edge.

2. In the second configuration the 1PPmS output of the ESAT-2000 GPS, at the end of the usual path underground is sent back to the external labor-atory, where it is compared with the 1 PPS signal, taking as a reference the middle height of the rising edge.

The used optoelectronic chain is kept identical in the two cases by simply swapping the receiver and the transmitter between the two locations. Further-more the jitter of the phase difference between the 1PPS and the 1PPmS outputs of the ESAT-2000 GPS receiver was checked to be negligible (< 0.25 ns).

3 Brief description of ICARUS

The ICARUS T600 detector consists of a large cryostat split into two identical, adjacent modules with internal dimensions 3.6 x 3.9 x 19.6 m3 filled with about 760 tons of ultra-pure liquid Argon [5-7]. Each module houses two TPCs separated by a common cathode and an electric field (ED = 500 V/cm). There are three parallel planes of wires, 3 mm apart with lengths up to 9 m, fac-ing the drift volume 1.5 m long. By appropriate voltage biasing, the first two planes provide signals in a non-destructive way. The third plane collects the ionization charge. There are 53248 channels in total. Wires are oriented on each plane at a different angle (0°, ±60°) with respect to the horizontal direction. Combining the wire coordinate on each plane at a given drift time, a three-dimensional image of the ionizing event is reconstructed. A remarkable resolu-tion of about 1 mm3 is uniformly achieved over the whole detector active vol-ume (~340 m3 corresponding to 476 t).

6

The scintillation light produced by ionizing events in the LAr-TPC is recorded with 74 photomultipliers (PMT) of 8 inches diameter. The PMT’s are organized in arrays located behind the four wire chambers (1L, 1R, 2L, 2R). The sums of the signals from the PMT arrays are used for the trigger and in order to locate the event within the drift volume. The scintillation decay time from LAr has two distinct components. The fast component (6 ns) records the early de-tectable photons within 1 ns from the ionization process. The trigger threshold at about 100 photoelectrons detects events with energy deposition as low as few hundred MeV with full efficiency. CNGS neutrinos are recorded within a coin-cidence between an “Early Warning Signal” of proton extraction from CERN and the PMT signals.

In the present measurement, the PMT readout has been equipped with an additional PMT-DAQ system based on three 2-channel, 8-bit, 1-GHz AGILENT AC240 digitizer boards, derived from the DAQ developed for the WArP experiment [16]. The PMT signals are continuously read out and stored in a memory buffer of a depth of 8 kB/channel, sampled at 1 GHz. At each CNGS trigger, additional data are readout and stored in the second local memory buffer. The content of all buffers is then transferred to the ICARUS da-ta storage for a time interval of 1400 µs.

The signal waveforms from the four PMT-Sums, integrated with a fast CANBERRA 2005 preamplifier, are recorded. The absolute time of the LNGS PPmS signal and its related coding are also recorded on additional channels. All channels are synchronized at the level of a few picoseconds. The time interval between the PMT-Sums and the PPmS signals allows the determination of the absolute time of the scintillation light pulse in the T600 detector within few ns precision. The LNGS time is referred to the half height of the PPmS leading edge (as in the calibration procedure). The time of the PMT-Sums is defined as the onset of the related signal, corresponding to the arrival time of the earliest scintillation photons.

Several delay corrections have been included in order to measure the neutrino arrival time. The propagation time of the scintillation light signals from the PMT’s to the AC240 boards include (1) the transit time within the PMT’s (~ 75 ns), (2) the overall cabling (~ 44 m) and (3) the delay through the signal adders and the preamplifier. The values are 299, 293, 295, 295 ns for chambers 1L, 1R, 2L, 2R respectively. The whole chain has been measured with the help of a laser diode. The associated uncertainty (± 5.5 ns) includes the vari-ations in the PMT transit time due to different biasing voltages and slight dif-ferences in cable lengths.

In addition, for each event, the distance of the event from the closest PMT and the position of the interaction vertex along the ~18 m of the detector length have been evaluated. The ICARUS upstream wall position has been used

7

as a reference coordinate for the neutrino time of flight. Both corrections have been deduced from the event topology in the detector through visual scanning. They are measurable with an accuracy better than 1 ns. Events in the standard ICARUS DAQ and the new PMT-DAQ have been associated through their common absolute time stamp.

Finally, the expected time of flight for v = c from the BCT position at CERN and the T600 upstream wall is (2439098 ± 1.5) ns (including the 2.2 ns contribution due to earth rotation). The overall distance of the CERN beam origin to ICARUS is (55.7 ± 0.5) m shorter than for OPERA.

4 Data analysis.

ICARUS started data taking with the CNGS low intensity bunched beam on October 27th, 2011. Unfortunately, due to an undetected time shift of 2 ms of the Early Warning Signal information with respect to the actual CERN-SPS pro-ton extraction time, the ICARUS DAQ trigger gate was out of time, resulting in empty events.

The problem was observed and settled on October 31st and, till Novem-ber 6th, the ICARUS T600 detector collected 7 beam-associated events, consistent with the CNGS delivered neutrino flux of 2.2 x 1016 p.o.t.

The events consist of three neutrino interactions (two CC and one NC) with the vertex contained within the ICARUS active volume and four addition-al through going muons generated by neutrinos interactions in the upstream rock. One of the two CC events and the NC one are shown respectively in Fig-ure 2a and Figure 2b.

Table 1 describes in detail the timing of each of the 7 events. The table is divided in the following sections: (1) properties of the ICARUS events; (2) CERN related data; (3) LNGS related data; (4) the time difference between the light and neutrino events.

As shown in Figure 1 and in Table 1, the proton transit time at the BCT (TSTART) in absolute GPS time base is obtained from the CERN proton extraction time plus fixed and variable corrections: TSTART = TCERN + δc1 + δc2 + D1 + δc3 + δc4 + δc5 + δc6, where D1 = -99216 ns (overall offset between CERN and GPS time bases), δc3 = 10078 ± 2 ns, δc4 = 27 ± 1 ns, δc5 = -580 ± 5 ns are the fixed de-lays. The event time in ICARUS (TSTOP) in absolute GPS time base is obtained from the LNGS distributed absolute time plus fixed and variable corrections: TSTOP = TLNGS + δl1 + δl2 - δl3 + δl4 - δl5 - δl6 - δl7 + D1, where the fixed delays D1 is 42037 ± 1.3 ns. The actual neutrino time of flight is calculated from TSTOP - TSTART accounting for the additional time related to the nearest proton bunch. The difference δt = tofς - tofν between the expected time of flight based on speed

8

of light (tofC = 2439098 ns) and the arrival time of neutrino in the ICARUS de-tector is shown in the last row.

The average δt value of the 7 events is + 0.3 ns with an r.m.s. of 10.5 ns and an estimated systematic error of ~9 ns, obtained from combining in quadra-ture all previously quoted uncertainties. Combining the 7 events compatibly with a common value of TSTOP - TSTART, the statistical error of the average is

€

10.5 7 = 4.0ns .

5 Conclusions

The expected time of flight difference between the speed of light from CERN to ICARUS and the actual position of the vertex of the LAr-TPC events has been neatly analysed. The result is compatible with the simultaneous arri-val of all the 7 events with the speed of light and not compatible with respect to the result reported by OPERA [1].

6 Acknowledgements.

The ICARUS Collaboration acknowledges the fundamental contribution of INFN to the construction and operation of the experiment. The Polish groups acknowledge the support of the Ministry of Science and Higher Education in Poland, including project 637/MOB/2011/0 and grant number N N202 064936. Finally we gratefully acknowledge the contribution of CERN, in particular the CNGS staff, for the very successful operation of the neutrino beam facility.

7 References [1] T. Adam et al. [OPERA Collaboration], arXiv:1109.4897. [2] P. Adamson et al. [MINOS Collaboration], Phys. Rev. D 76 (2007) 072005

[arXiv:0706.0437]. [3] G. R. Kalbfleisch, N. Baggett, E. C. Fowler and J. Alspector, Phys. Rev.

Lett. 43 (1979) 1361. [4] A.G. Cohen, and S.L. Glashow, Phys. Rev. Lett., 107, 181803 (2011).

[5] C. Rubbia, “The Liquid-Argon Time Projection Chamber: A New Con-cept For Neutrino Detector”, CERN-EP/77-08 (1977).

[6] S. Amerio et al., Nucl. Instr. Meth. A527 (2004) 329. [7] C. Rubbia et al., JINST 6 (2011) P07011. [8] M. Antonello et al. [ICARUS Collaboration], arXiv:1110.3763v1,

arXiv:1110.3763v3, (Submitted to Physics Letters, February 25, 2012).

9

[9] R. M. Bionta et al. [IMB Collaboration], Phys. Rev. Lett. 58 (1987) 1494. [10] E. N. Alekseev, L. N. Alekseeva, I. V. Krivosheina and V. I. Volchenko,

Phys. Lett. B 205 (1988) 209. [11] K. Hirata et al. [KAMIOKANDE-II Collaboration], Phys. Rev. Lett. 58

(1987) 1490. [12] J. R. Ellis, N. Harries, A. Meregaglia, A. Rubbia and A. Sakharov, Phys.

Rev. D 78 (2008) 033013 [arXiv:0805.0253]. [13] P. Alvarez and J. Serrano, CERN BE-CO-HT Internal Note, (Oct. 16,

2011). [14] Master clock GPS 2000, http://www.esat.it/EN/default.htm, M. Am-

brosio, et al., Phys. Rev. D 62 (2000) 052003. [15] M. Ambrosio et al., The MACRO detector at Gran Sasso, Nucl. Instr.

Meth. A 486 (2002) 663. [16] R. Acciarri et al., Journal of Phys.: Conf. Series 308 (2011) 012005, and

references therein.

10

Tabl

e 1.

Eve

nts c

olle

cted

with

CN

GS

bunc

hed

beam

. The

act

ual n

eutr

ino

time

of fl

ight

is c

alcu

late

d fr

om T

STO

P - T

STA

RT a

c-co

untin

g fo

r th

e ad

ditio

nal t

ime

rela

ted

to th

e ne

ares

t pro

ton

bunc

h. T

he d

iffer

ence

δt =

tofc

- tofν

with

res

pect

to th

e ex

pect

ed

time

of fl

ight

bas

ed o

n th

e sp

eed

of li

ght (

tofc

= 24

3909

8 ns

) is s

how

n in

the

last

row

. For

det

ails

we

refe

r to

the

text

.

(*) T

he v

alue

for e

vent

#1

has a

larg

er u

ncer

tain

ty o

f abo

ut 4

ns (

abou

t the

dou

ble t

han

that

of t

he o

ther

even

ts),

beca

use o

f the

smal

ler si

ze o

f th

e PM

T sig

nal.

Even

t #

1 2

3 4

5 6

7 G

ener

al p

rope

rtie

s of t

he e

vent

Dat

e 31

-Oct

1-

Nov

1-

Nov

2-

Nov

2-

Nov

2-

Nov

4-

Nov

Ti

me

(UTC

+1)

08:4

1:22

.554

03

:57:

00.9

54

09:1

1:56

.154

02

:49:

16.5

56

11:1

8:51

.356

16

:53:

41.7

56

23:3

1:27

.356

R

un n

umbe

r 10

949

1094

9 10

949

1095

0 10

951

1095

1 10

956

Even

t Num

ber

338

1247

18

85

1053

91

80

2 77

3 Ty

pe o

f eve

nt

Mu-

rock

N

u-N

C

Nu-

CC

M

u-ro

ck

Nu-

CC

M

u-ro

ck

Mu-

rock

TC

P ch

ambe

r (PM

T ar

ray)

1R

(1L)

1R

(1L)

1L

(1L)

2L

(2R

) 1L

(1L)

2L

(2R

) 2L

(2R

)

C

ER

N re

late

d da

ta

C

ERN

ext

ract

ion

time,

TC

ERN (C

ERN

tim

e ba

se, n

s)

1330

04

1133

99

1141

72

1310

46

1168

52

1170

40

1183

40

1st C

ERN

tim

e lin

k co

rrec

tion,

δc1

(ns)

24

43

2457

24

64

2487

25

00

2507

25

58

2nd C

ERN

tim

e lin

k co

rrec

tion,

δc2

(ns)

86

603

8659

0 86

585

8656

4 86

556

8653

7 86

500

BC

T de

lay

(firs

t bun

ch), δc

6 (n

s)

6047

60

44

6049

60

55

6050

60

41

6046

Pr

oton

tran

sit t

ime

at B

CT,

TST

AR

T (G

PS ti

me

base

, ns)

13

8406

11

8799

11

9579

13

6461

12

2267

12

2434

12

3753

LN

GS

rela

ted

data

LNG

S di

strib

uted

tim

e, T

LNG

S (LN

GS

time

base

, ns)

30

0000

0 30

0000

0 30

0000

0 30

0000

0 30

0000

0 30

0000

0 30

0000

0 1st

LN

GS

time

link

corr

ectio

n, δ

l1 (n

s)

-731

6 -7

317

-732

1 -7

318

-731

3 -7

312

-732

3 2nd

LN

GS

time

link

corr

ectio

n, δ

l2 (n

s)

7035

70

30

7062

70

29

7064

70

60

7041

LN

GS

time

on A

C24

0, δ

l3 (n

s)

4716

02

4911

67

4898

89

4740

31

4872

31

4865

70

4862

96

PMT

time

on A

C24

0, δ

l4 (n

s)

8196

(*)

8193

81

94

8190

81

85

8204

82

12

PMT

cabl

e de

lay,

δl5

(ns)

29

9 29

9 29

9 29

5 29

9 29

5 29

5 V

erte

x po

sitio

n co

rrec

tion,

δl6

(ns)

0

40

44

16

28

5 1

PMT

posi

tion

corr

ectio

n, δ

l7 (n

s)

12

11

5 13

4

13

13

Even

t tim

e in

ICA

RU

S, T

STO

P (G

PS ti

me

base

, ns)

25

7803

0 25

5842

1 25

5973

0 25

7557

8 25

6240

6 25

6310

1 25

6335

7

N

eutr

ino

time-

of-f

light

cal

cula

tion

T S

TOP -

TST

AR

T (n

s)

2439

632

2439

622

2440

151

2439

117

2440

139

2440

667

2439

604

Nea

rest

pro

ton

bunc

h 2

2 3

1 3

4 2

Bun

ch re

late

d ad

ditio

nal t

ime

(ns)

52

4 52

4 10

48

0 10

48

1572

52

4 N

eutri

no ti

me

of fl

ight

(tofν,

ns)

24

3910

4 24

3909

8 24

3910

3 24

3911

7 24

3909

1 24

3909

5 24

3908

0 Ti

me

diff

eren

ce w

.r.t.

expe

ctat

ion

(δt =

tofc

- to

fν, n

s)

-6

0 -5

-1

9 +7

+3

+1

8

11

Figu

re 1

. Gen

eral

layo

ut o

f the

CER

N-L

NG

S tim

e-lin

k fo

r neu

trin

o tim

e of

flig

ht m

easu

rem

ent.

All

timin

g de

lays

are

show

n.

15 March 2012

Figure 2. (a) CC event in the chamber 1L. (b) NC event in the chamber 1R, as

visible in the LAr collection view. The actual distances of the vertex from the upstream wall of the detector are indicated. The spontaneously in-duced signal of the closest PMT induced to the signals from the LAr col-lecting wires is also visible.

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Figure 3. Time distribution in ns of the difference δt between the neutrino time

of flight in the ICARUS LAr-TPC as recorded on the closest PMT signal and the expectation based on speed of light as measured in ICARUS. Events are compatible with Lorentz invariance, which requires a negligi-ble value δt ≈ 0. The r.m.s. value of the average of the recorded distribu-tion is

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δt = 0.3 ± 4.0stat ± 9.0syst( )ns. The OPERA result is also shown as a comparison, with the different values

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δt = 57.8 ± 7.8stat −5.9+8.3( )'syst( ) ns .